HR: 1340h
AN: SM43B-1229    [Abstracts]
TI: Near Simultaneous Observations of the Aurora From FUV, Particle and Photometric Instruments on DMSP-F16, TIMED, and IMAGE
AU: * Hecht, J H
EM: james.hecht@aero.org
AF: Space Science Applications Laboratory, The Aerospace Corp, MS M2-259 PO Box 92957, Los Angeles, CA 90009 United States
AU: Strickland, D J
EM: dstrick@cpi.com
AF: Computational Physics Inc, 8001 Braddock Rd Ste 210, Springfield, VA 22151 United States
AU: Knight, H K
EM: hknight@cpi.com
AF: Computational Physics Inc, 8001 Braddock Rd Ste 210, Springfield, VA 22151 United States
AU: Kochenash, A J
EM: ajk@cpi.com
AF: Computational Physics Inc, 8001 Braddock Rd Ste 210, Springfield, VA 22151 United States
AU: Zhang, Y
EM: yongliang.zhang@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Lab., MP3-W171 11100 Johns Hopkins Rd., Laurel, MD 20723 United States
AU: Morrison, M D
EM: daniel.morrison@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Lab., MP3-W171 11100 Johns Hopkins Rd., Laurel, MD 20723 United States
AU: Paxton, L J
EM: larry.paxton@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Lab., MP3-W171 11100 Johns Hopkins Rd., Laurel, MD 20723 United States
AU: Mende, S B
EM: mende@ssl.berkeley.edu
AF: University California Berkeley, Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Frey, H U
EM: hfrey@ssl.berkeley.edu
AF: University California Berkeley, Space Sciences Lab, 7 Gauss Way, Berkeley, CA 94720 United States
AU: Burke, W J
EM: william.burke2@hanscom.af.mil
AF: Air Force Research Laboratory, (VSBXP), 29 Randolph Rd, Hanscom AFB, MA 01731-3010 United States
AU: Rich, F J
EM: frederick.rich@hanscom.af.mil
AF: Air Force Research Laboratory, (VSBXP), 29 Randolph Rd, Hanscom AFB, MA 01731-3010 United States
AB: With the launch of DMSP F16 there are now three FUV remote sensing instruments which measure auroral emissions originating from the impact of electrons and protons on atmospheric constituents. These instruments are the FUV cameras on IMAGE which generally observes from HEO (approximately 7 Re apogee), the GUVI instrument on TIMED, and the SSUSI instrument on F16 which are in LEO. The Image cameras measure the OI (1356) emission, Ly-alpha, and the N2 LBH bands. GUVI, although a spectrograph, generally produces images in 5 colors (Ly-alpha, OI(1304), OI(1356), LBH-short and LBH-long). SSUSI is at a slightly higher altitude and includes a spectrograph that is essentially identical to the GUVI instrument. All these data can be used to determine the energetics of the auroral precipitation using algorithms. Unique to DMSP are two other instruments, J5, a particle sensor which measures electron and proton fluxes from 30 eV to 30 keV, and as part of SSUSI, a multi-channel photometer measuring two emission (N2+(4278) and OI(6300)) which are often used in ground-based applications to measure auroral particle energetics. In a companion paper (Knight et al.) a statistical analysis is given on how well the SSUSI spectrograph derived energy flux, Q, is compared to the J5 measured Q. In this paper we present results for several individual events where data can be obtained from most or all of these five instruments. The results for Q and the average energy of the particle flux are compared. In particular, we look at whether there is any significant difference between these derived quantities during proton-dominated and electron-dominated aurorae.
DE: 0310 Airglow and aurora
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005